Overview of the Dark Energy Spectroscopic Instrument

Martini, Paul; Bailey, S.; Besuner, Robert; Doel, P.; Edelstein, Jerry; Eisenstein, Daniel; Flaugher, B.; Gutiérrez, G.; Harris, S.; Honscheid, K.; Jelinsky, Patrick; Joyce, Richard; Kent, Stephen M.; Levi, M. E.; Prada, Francisco; Poppett, Claire; Rabinowitz, D.; Rockosi, Constance M.; Sas, Laia Cardiel; Schlegel, David J.; Schubnell, M.; Sharples, R. M.; Silber, Joseph; Sprayberry, David

doi:10.1117/12.2313063

Cited by 30 publications

(13 citation statements)

References 12 publications

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“…Furthermore, researchers have scoured all-sky images for concetrations of LRGs and other red galaxies to identify groups and clusters to z ∼ 1 (Rykoff et al 2016). Imaging surveys on both sides of the planet provide millions of LRGs across the sky and several million will have have spectroscopically measured redshifts by 2020 (Martini et al 2018). For precisely localized FRBs with redshifts, a sample of ∼ 50 events at z ∼ 1 (i.e.…”

Section: Groups and Clustersmentioning

confidence: 99%

Probing Galactic Halos with Fast Radio Bursts

Prochaska

Zheng

2019

Monthly Notices of the Royal Astronomical Society

212

247

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The precise localization (< 1 ) of multiple fast radio bursts (FRBs) to z > 0.1 galaxies has confirmed that the dispersion measures (DMs) of these enigmatic sources afford a new opportunity to probe the diffuse ionized gas around and in between galaxies. In this manuscript, we examine the signatures of gas in dark matter halos (aka halo gas) on DM observations in current and forthcoming FRB surveys. Combining constraints from observations of the high velocity clouds, O vii absorption, and the DM to the Large Magellanic Cloud with hydrostatic models of halo gas, we estimate that our Galactic halo will contribute DM MW,halo ≈ 50 − 80pc cm −3 from the Sun to 200 kpc independent of any contribution from the Galactic ISM. Extending analysis to the Local Group, we demonstrate that M31's halo will be easily detected by high-sample FRB surveys (e.g. CHIME) although signatures from a putative Local Group medium may compete. We then review current empirical constraints on halo gas in distant galaxies and discuss the implications for their DM contributions. We further examine the DM probability distribution function of a population of FRBs at z 0 using an updated halo mass function and new models for the halo density profile. Lastly, we illustrate the potential of FRB experiments for resolving the baryonic fraction of halos by analyzing simulated sightlines through the CASBaH survey. All of the code and data products of our analysis are available at https://github.com/FRBs.

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Section: Groups and Clustersmentioning

confidence: 99%

Probing Galactic Halos with Fast Radio Bursts

Prochaska

Zheng

2019

Monthly Notices of the Royal Astronomical Society

212

247

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“…The CCD sensors used by CONNIE were developed by the experiment in collaboration with the LBNL Micro Systems Labs [31]. These detectors are a spin-off from the fully depleted thick detectors that were originally designed to give astronomical instruments such as DECam [32] and DESI [33] extended sensitivity in the near-infrared region. CONNIE increased the CCD thickness to 675 µm.…”

Section: A Ccd Sensorsmentioning

confidence: 99%

Exploring low-energy neutrino physics with the Coherent Neutrino Nucleus Interaction Experiment

Aguilar-Arevalo¹,

Bertou²,

Bonifazi³

et al. 2019

Phys. Rev. D

106

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The Coherent Neutrino-Nucleus Interaction Experiment (CONNIE) uses low-noise fully depleted charge-coupled devices (CCDs) with the goal of measuring low-energy recoils from coherent elastic scattering (CEνNS) of reactor antineutrinos with silicon nuclei. This standard model process has not yet been observed at recoil energies below 20 keV. We report here the first results of the detector array deployed in 2016, with an active mass of 73.2 g (12 CCDs), which is operating at a distance of 30 m from the core of the Angra 2 nuclear reactor, with a thermal power of 3.8 GW. A search for neutrino events is performed by comparing data collected with reactor on (2.1 kg-day) and reactor off (1.6 kg-day). The results show no excess in the reactor-on data, reaching the world record sensitivity down to recoil energies of about 1 keV (0.1 keV electron-equivalent). A 95% confidence level limit for new physics is established at an event rate of 40 times the one expected from the standard model at this energy scale. The results presented here provide a new window to the low-energy neutrino physics, which allows one to explore for the first time the lowest energies accessible through the CEνNS with antineutrinos from nuclear reactors.

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“…The 8.4-m Rubin imaging telescope (formerly the LSST) will shortly start operation with a 3.2 gigapixel silicon imager array, sampling a 3.5°, 0.64-m diameter field with 0.2 arcsec (10 µm) pixels [ 7 ]. Spectroscopic follow-up will use the 3.8-m Mayall telescope now equipped with the DESI multi-object spectrograph, which obtains simultaneously spectra of 5000 objects chosen from a 3.2° field of view [ 8 ]. Larger telescopes for multi-object spectroscopy are being designed, for example, 6.5-m and 20 m telescopes with 3° field to accommodate 10 000 positionable 1.2 arcsec fibres [ 9 ].…”

Section: Introductionmentioning

confidence: 99%

A 20 m wide-field diffraction-limited telescope

Eads

Angel

2020

Phil. Trans. R. Soc. A.

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A 20 m space telescope is described with an unvignetted 1° field of view—a hundred times larger in area than fields of existing space telescopes. Its diffraction-limited images are a hundred times sharper than from wide-field ground-based telescopes and extend over much if not all the field, 40 arcmin diameter at 500 nm wavelength, for example. The optical system yielding a 1°, 1.36 m diameter image at f/3.9 has relatively small central obscuration, 9% by area on axis, and is fully baffled. Several carousel-mounted instruments can each access directly the full image. The initial instrument complement includes a 400 gigapixel silicon imager with 2 µm pixels (0.005 arcsec), and a 60 gigapixel HgCdTe imager with 5 µm pixels (0.012 arcsec). A multi-object spectrograph with 10 000 fibres will allow spectroscopy with 0.02 arcsec resolution. Direct imaging and spectroscopy of exoplanets can take advantage of the un-aberrated, on-axis image (5 nm RMS wavefront error). While this telescope could be built for operation in free space, a site accessible to a human outpost at the Moon's south pole would be advantageous, for assembly and repairs. The lunar site would allow also for the installation of new instruments to keep up with evolving scientific priorities and advancing technology. Cooling to less than 100E K would be achieved with a surrounding cylindrical thermal shield. This article is part of a discussion meeting issue ‘Astronomy from the Moon: the next decades’.

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Overview of the Dark Energy Spectroscopic Instrument

Cited by 30 publications

References 12 publications

Probing Galactic Halos with Fast Radio Bursts

Probing Galactic Halos with Fast Radio Bursts

Exploring low-energy neutrino physics with the Coherent Neutrino Nucleus Interaction Experiment

A 20 m wide-field diffraction-limited telescope

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